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HR 5553: Revision history


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  • curprev 01:1301:13, 17 November 2021 Urhixidur talk contribs 12,531 bytes +241 {{cite journal |doi=10.1111/j.1365-2966.2004.07588.x | title=Kinematics of chromospherically active binaries and evidence of an orbital period decrease in binary evolution | journal=Monthly Notices of the Royal Astronomical Society | volume=349 | issue=3 | pages=1069–1092 | bibcode=2004MNRAS.349.1069K |arxiv = astro-ph/0404219 | last1=Karataș | first1=Yüksel | last2=Bilir |first2=‪Selçuk | last3=Eker |first3=Zeki | last4=Demircan |first4=Osman | last5=Liebert |first5=James undo

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  • curprev 23:4823:48, 3 October 2019 99.230.229.254 talk 8,976 bytes −2 semi-major axis is 0.52 AU minimum (Nidever et al 2002); measurement of the spectroscopic separation to 16.5 mas falsifies the parallax and consequently the distance to the system, not the mass and semi-major axis. see the discussion undo

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